^1,2,3Min Li,^2,4Zhaohuan Zhu,⁵Shichun Huang,⁶Ning Sui,⁷Michail I. Petaev,^2,4Jason H. Steffen
The Astrophysical Journal 958, 58 Open Access Link to Article [DOI 10.3847/1538-4357/acfb02]
¹College of Physics, Jilin Normal University, Siping, Jilin 136000, People’s Republic of China
²Department of Physics and Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy., Las Vegas, NV 89154, USA
³Key Laboratory of Functional Materials Physics and Chemistry of the Ministry of Education, Jilin Normal University, Changchun, Jilin 130103, People’s Republic of China
⁴Nevada Center for Astrophysics, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy., Las Vegas, NV 89154, USA
⁵Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, 1621 Cumberland Ave., Knoxville, TN 37996, USA
⁶College of Physics, Jilin University, Changchun, Jilin 130012, People’s Republic of China
⁷Department of Earth and Planetary Sciences, Harvard University, 20 Oxford St., Cambridge, MA 02138, USA

The temperatures of observed protoplanetary disks are not sufficiently high to produce the accretion rate needed to form stars, nor are they sufficient to explain the volatile depletion patterns in CM, CO, and CV chondrites and terrestrial planets. We revisit the role that stellar outbursts, caused by high-accretion episodes, play in resolving these two issues. These outbursts provide the necessary mass to form the star during the disk lifetime and provide enough heat to vaporize planet-forming materials. We show that these outbursts can reproduce the observed chondrite abundances at distances near 1 au. These outbursts would also affect the growth of calcium-aluminum-rich inclusions and the isotopic compositions of carbonaceous and noncarbonaceous chondrites.